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首页> 外文期刊>International journal of modern physics, D. Gravitation, astrophysics, cosmology >Dark energy in Horndeski theories after GW170817: A review
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Dark energy in Horndeski theories after GW170817: A review

机译：GW170817后Horndeski理论中的黑暗能量：审查

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The gravitational wave (GW) event GW170817 from a binary neutron star merger together with the electromagnetic counterpart showed that the speed of GWs c(t) is very close to that of light for the redshift z < 0.009. This places tight constraints on dark energy models constructed in the framework of modified gravitational theories. We review models of the late-time cosmic acceleration in scalar-tensor theories with second-order equations of motion (dubbed Horndeski theories) by paying particular attention to the evolution of dark energy equation of state and observables relevant to the cosmic growth history. We provide a gauge-ready formulation of scalar perturbations in full Horndeski theories and estimate observables associated with the evolution of large-scale structures, cosmic microwave background and weak lensing by employing a so-called quasi-static approximation for the modes deep inside the sound horizon. In light of the recent observational bound of c(t), we also classify surviving dark energy models into four classes depending on different structure-formation patterns and discuss how they can be observationally distinguished from each other. In particular, the nonminimally coupled theories in which the scalar field phi has a coupling with the Ricci scalar R of the form G(4)(phi) R, including f(R) gravity, can be tightly constrained not only from the cosmic expansion and growth histories but also from the variation of screened gravitational couplings. The cross-correlation of integrated Sachs-Wolfe signal with galaxy distributions can be a key observable for placing bounds on the relative ratio of cubic Galileon density to total dark energy density. The dawn of GW astronomy will open up a new window to constrain nonminimally coupled theories further by the modified luminosity distance of tensor perturbations.
机译：来自二进制中子星的引力波（GW）事件GW170817与电磁对应物的合并显示，GWS C（T）的速度非常接近Redshift Z <0.009的光的光。这对修改的引力理论框架构建的暗能模型来说紧张的限制。我们通过特别注意状态和与宇宙增长历史相关的暗能方程的演变，用二阶方程（被称为Horndeski理论）的二阶方程来审查标量动作（被称为Horndeski理论）中的尺寸宇宙加速模型。我们在全霍恩斯基理论中提供了一项规范的标量扰动，并通过采用所谓的准静态近似为声音内部的模型来实现与大规模结构，宇宙微波背景和弱透镜相关的可观察到。地平线。鉴于最近的C（t）的观察结果，我们还根据不同的结构形成模式将幸存的暗能量模型分为四个类别，并讨论如何彼此观察地区分它们。特别地，标量场PHI具有与形式G（4）（PHI）R的RICCI标量R耦合的非体于耦合理论，包括F（R）重力，不仅可以严格地限制宇宙扩展和生长历史，但也来自筛选的引力联轴器的变化。具有星系分布的集成Sachs-Wolfe信号的互相关可以是可观察到在立方伽利罗琴密度的相对比上的界限到总暗能密度的键。 GW天​​文学的曙光将打开一个新的窗口，以通过张解扰动的修改亮度距离进一步约束非体于耦合的理论。

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